研究期間：10108~10207;It is generally believed that the hard X-ray (HXR) emission is a critical characteristic of energy release in the impulsive phase of solar flare. The chromospheric HXR kernels are regarded as the footpoints of newly reconnected magnetic field lines. It is thought to be associated with the acceleration process in the corona, collision process in the chromosphere, and the transportation process between the chromosphere and corona. We believe that the properties of HXR emissions in the impulsive phase of solar flare strongly depend on the ambient plasma and magnetic field conditions in the coronal reconnection or acceleration region. Since the magnetic field in the solar corona is unavailable to be directly measured, it is important to investigate the influence of solar coronal magnetic fields on the energy storage and release. The purpose of this study is to qualitatively and quantitatively analyze the associated physical quantities to understand the mechanism of reconnection and acceleration in solar flares, based on the coronal magnetic fields extrapolated by a non-linear force-free field model, the HXR imaging and spectrum analyses, and high-resolution transversal and longitudinal magnetic field observations.
